Science development study for the Atacama Large Aperture Submillimeter Telescope (AtLAST): Solar and stellar observations

Observations at (sub-)millimeter wavelengths offer a complementary perspective on our Sun and other stars, offering significant insights into both the thermal and magnetic composition of their chromospheres. Despite the fundamental progress in (sub-)millimeter observations of the Sun, some important aspects require diagnostic capabilities that are not offered by existing observatories. In particular, simultaneously observations of the radiation continuum across an extended frequency range would facilitate the mapping of different layers and thus ultimately the 3D structure of the solar atmosphere. Mapping large regions on the Sun or even the whole solar disk at a very high temporal cadence would be crucial for systematically detecting and following the temporal evolution of flares, while synoptic observations, i.e., daily maps, over periods of years would provide an unprecedented view of the solar activity cycle in this wavelength regime. As our Sun is a fundamental reference for studying the atmospheres of active main sequence stars, observing the Sun and other stars with the same instrument would unlock the enormous diagnostic potential for understanding stellar activity and its impact on exoplanets. The Atacama Large Aperture Submillimeter Telescope (AtLAST), a single-dish telescope with 50m aperture proposed to be built in the Atacama desert in Chile, would be able to provide these observational capabilities. Equipped with a large number of detector elements for probing the radiation continuum across a wide frequency range, AtLAST would address a wide range of scientific topics including the thermal structure and heating of the solar chromosphere, flares and prominences, and the solar activity cycle. In this white paper, the key science cases and their technical requirements for AtLAST are discussed.

Despite the fundamental progress in (sub-)millimeter observations of the Sun, some important aspects require diagnostic capabilities that are not offered by existing observatories.In particular, simultaneously observations of the radiation continuum across an extended frequency range would facilitate the mapping of different layers and thus ultimately the 3D structure of the solar atmosphere.Mapping large regions on the Sun or even the whole solar disk at a very high temporal cadence would be crucial for systematically detecting and following the temporal evolution of flares, while synoptic observations, i.e., daily maps, over periods of years would provide an unprecedented view of the solar activity cycle in this wavelength regime.
As our Sun is a fundamental reference for studying the atmospheres of active main sequence stars, observing the Sun and other stars with the same instrument would unlock the enormous diagnostic potential for understanding stellar activity and its impact on exoplanets.
The Atacama Large Aperture Submillimeter Telescope (AtLAST), a single-dish telescope with 50m aperture proposed to be built in the Atacama desert in Chile, would be able to provide these observational

Introduction
The continuum radiation emitted by the Sun at millimeter wavelengths originates from the chromosphere, the layer of the solar atmosphere located between the photosphere and the corona.The thermal and magnetic structure of the chromosphere is complex and highly dynamic with a plethora of physical processes at work, many of which induce notable deviations from equilibrium conditions (for example in the ionisation state of hydrogen).The largest features like filaments can span substantial fractions of the solar diameter (∼30'), followed by Active Regions (often a few arcminutes), and magnetic network cells as the chromospheric imprints of supergranulation cells (20" -60").Sunspots, including the penumbra, have diameters of typically 30" but occasionally up to ∼ 1', whereas the atmosphere in the Quiet Sun regions exhibits spatial scales of 1-2" and below.It is expected that there is small-scale structure even smaller than ∼ 0.1" scales resolved by modern 4m-class optical solar telescopes (Quintero Noda et al., 2022;Rimmele et al., 2020).Likewise, the temporal scales range from about a month for one solar rotation, days for the evolution of sunspots, down to minutes and seconds for small-scale and energetic phenomena.
Consequently, observing the chromosphere and characterising the physical mechanisms that govern this dynamic environment is challenging.So far, there were only a few suitable diagnostic tools available to examine the plasma conditions in the chromosphere such as the spectral lines of singly ionized calcium (Ca II) and magnesium (Mg II) as well as the Hα line.The interpretation of observations in these spectral lines and deriving the physical properties of the plasma in the mapped atmospheric regions is complicated and limited by the complex line formation mechanisms that involve non-local thermodynamic equilibrium effects.The situation is better for the millimeter continuum radiation, which is assumed to be formed mostly under local equilibrium conditions so that the measured brightness temperature should be closely related to the local plasma temperature.Although available telescopes for millimeter wavelengths made notable contributions to solar physics in the past (e.g., Kundu 1959; Loukitcheva et al., 2014;Trottet et al., 2011, and references therein), they did not have sufficient spatial resolution for resolving the small spatial scales in the solar chromosphere until the Atacama Large Millimeter/submillimeter Array (ALMA) started regular observations of the Sun in 2016 (Bastian, 2002;Karlický et al., 2011;Shimojo et al., 2017b;White et al., 2017).It should also be noted that the chromosphere evolves on timescales well below 1 min, which meant that meaningful observations are restricted to very short integration times essentially leading to snapshot imaging.Techniques like Earth rotation synthesis or combining observations in different array configurations are not viable for solar observations.The high spatial and temporal resolution and also the prospects for utilising polarisation measurements for measuring magnetic fields in the solar chromosphere make (sub-)millimeter telescopes very powerful tools for investigating the solar chromosphere and thus contributing to the solution of many open questions (see Wedemeyer et al., 2016, and references therein).
It should also be noted that the continuum radiation received at a certain frequency mostly originates from a narrow layer in the solar atmosphere with the mapped height range depending on the used receiver band.Observations of the Sun in different receiver bands thus map different layers in the Sun's atmosphere.Despite already large success of ALMA in advancing solar physics (e.g.Brajša 2021), there are important science cases that require different observational capabilities.One diagnostic limitation is that observations are limited to one narrow frequency band and therefore to one atmospheric layer at a time, while the solar atmosphere is a prime example of a dynamic, complex, and inherently 3D phenomenon.Meaningful observations must therefore be carried out strictly simultaneously with as many complementary diagnostics and in as many layers as technically possible.This capability could be offered by a large-aperture sub-millimeter facility telescope like the proposed Atacama Large Submillimeter Telescope (AtLAST Klaassen et al., 2020; Mroczkowski et al., 2023; Mroczkowski et al., 2024; Ramasawmy et al., 2022, http://atlast-telescope. org/).Despite an impressive aperture of 50 m, AtLAST would not reach the angular resolution achieved with an interferometric array like ALMA but compensate with other unique features such as a simultaneous wider frequency coverage, thus unlocking complementary science cases.AtLAST would thus have the potential to boost the impact of millimeter observations on solar physics beyond its current state.In this article, key science cases and observing strategies for solar observations with AtLAST are described.

Key science cases
The chromosphere is an integral part of the solar atmosphere and as such plays an important role in the transport of energy and matter.These are essential for understanding the heating of the corona, the origins of the solar wind, and the drivers of solar activity and space weather.There is a plethora of physical processes involved, which are entangled in complicated dynamic ways, rendering the understanding of the workings of our Sun a challenging undertaking.
As detailed in the sections below, AtLAST (Mroczkowski et al., 2024) opens up a new window to science cases that cannot be addressed with existing sub-mm telescopes.In addition, some solar science cases for ALMA (see Bastian et al., 2018;Wedemeyer et al., 2016, and references therein; see also Figure 1) and LLAMA (Lépine et al., 2021) are potential solar use cases for AtLAST, too, thus creating synergies between these observatories.These science cases concern the thermal structure of the solar atmosphere including the thermal structure of prominences and filaments, the related transport of energy and mass, and phenomena related to solar activity.In the following, the key science cases for AtLAST are highlighted.

Thermal structure and the atmospheric heating problem
One of the large open questions in solar physics is the coronal heating problem, which has been known since the late 1930s when observations of spectral lines due to elements in extremely high ionisation stages implied temperatures in excess of a million Kelvin in the corona (Edlén, 1943).As pointed out in the introduction, deriving the plasma properties in the outer solar atmosphere is difficult, which hampered identifying the processes responsible for the transport of the required energy into the corona.As a result, much of the coronal heating problem remains unsolved today.It should be noted that the Sun is not unique in this sense but rather serves as a reference for other stars that exhibit a corona, too, thus making the solar coronal heating problem relevant for late-type stars in general.
After decades of research, numerous processes have been identified that are capable of supplying the energy required to account for the high temperatures observed in the Sun.The focus has shifted towards determining which of these processes are most relevant and how exactly they transport and deposit energy.It is likely that a combination of different processes contributes to chromospheric/coronal heating, with their relative importance varying in different solar regions characterized by distinct magnetic field environments and activity levels, i.e. from Active Regions to Quiet Sun regions.Some processes provide continuous heating, while others, such as solar flares, produce a more variable and intermittent heating component due to their transient nature.Typically these phenomena are grouped into processes related to (i) magnetic reconnection/Ohmic heating and (ii) wave heating processes, specifically acoustic and magnetohydro-dynamic (MHD) waves.MHD waves, including Alfvén waves, can contribute to plasma heating by perturbing the magnetic field, leading to wave damping and the release of magnetic and kinetic energy, but, in turn, can also be excited by dynamic variations of magnetic field structures.The resulting heating is evident in phenomena like spicules observed at the solar limb.The multitude of possible heating mechanisms and their potential entanglement has made it challenging to determine which ones are predominant and how their contributions depend on the solar region type.In principle, identifying these mechanisms and understanding their contributions requires quantitative and precise measurements that capture the thermal, magnetic, and kinetic state of chromospheric plasma over time and in three spatial dimensions.AtLAST has the potential to provide such data.

Solar flares
AtLAST is poised to make significant contributions in addressing numerous unresolved inquiries pertaining to solar flares, a prominent conundrum within contemporary solar physics that continues to be a highly dynamic area of investigation.Although numerous intricacies remain shrouded in mystery, it is evident that solar flares manifest as a result of the dynamic reconfiguration and interconnection of magnetic fields within the solar atmosphere.Consequently, substantial amounts of energy previously stored within the magnetic field are explosively released during these events, manifesting as both radiation and high-energy particles.This emitted radiation encompasses the entire electromagnetic spectrum, spanning from gamma and X-rays to mm and radio waves.Solar flares can differ by orders of magnitude in strength, which is typically measured according to the emitted soft X-ray flux.The strongest solar flares ever documented released energy on the order of 10 32 ergs (Emslie et al., 2005) and are often accompanied by coronal mass ejections (CME) that can impact space weather with notable effects on Earth.The effects manifest themselves from beautiful aurorae to severe disturbances of power grids (like the Quebec blackout in 1989) and satellite infrastructure.As a recent example, we can mention the destruction of the majority of a batch of Starlink satellites due to solar activity (e.g.Dang et al., 2022).And yet, it cannot be ruled out that even stronger flares exceeding the Carrington event of 1859 could occur with disastrous consequences for our technology-dependent modern society.Such so-called super-flares are observed for other (solar-like) stars (Maehara et al., 2012) (see Section 2.5).The study of strong solar flares, to which AtLAST can contribute in new ways, is thus of utmost importance.
The occurrence rate of a flare is roughly related to the released energy, making the strongest events rare (although varying with the solar cycle) and the much weaker micro-and nano-flares more frequent and ubiquitous.The latter are therefore extremely important as potential contribution to the heating of the corona (see Section The mm and sub-mm data can uniquely address several key questions regarding solar flares (Fleishman et al., 2022).For example, in combination with other instruments for higher frequencies (see Section 3.4), the spectral coverage in the mid-IR to sub-mm range can help to unveil the thermal structure of the flaring atmosphere.Radiative-hydrodynamic (RHD) modelling of flares suggest that the emission at wavelengths longer than 50 µm is optically thick, and thus, the observed brightness temperature should directly provide estimates for the electron temperature at the emitting chromospheric layer (Simões et al., 2017).In Figure 2, we provide an example of the temporal evolution of a synthetic flare spectrum from RHD modelling.
Addressing these aspects with AtLAST would require high spectral, spatial and temporal resolution and preferably full polarisation, which then would allow for probing the dynamic thermal structure and magnetic structure of the solar atmosphere before, during, and after a flare with potentially ground-breaking insights.While already the thermal free-free radiation produced mostly due by electron-ion free-free absorption and H − free-free absorption (e.g.Heinzel & Avrett, 2012) contains essential information about the physical mechanisms behind flares, the non-thermal radiation component due to gyrosynchrotron and resonance processes would be essential for constraining the acceleration of charged particles, which is central to understanding flares.

Solar prominences
Multi-scale observations of solar prominences, i.e. extended structures in the solar atmosphere that stretch upward from the visible surface into the corona (Vial & Engvold, 2015), are another area where AtLAST can make a significant impact.The magnetic field in a prominence supports denser prominence plasma against gravity.The prominence material has a much lower temperature (around 10 4 K) while being surrounded by coronal plasma (around 10 6 K).Here, the prominence magnetic field provides the insulation, which allows the prominence plasma to cool radiatively.Prominences appear as bright when viewed above the solar limb but dark when viewed against the solar disk's brightness (when they are called filaments).Quiescent prominences can extend over a few hundred thousand kilometers, i.e. a significant fraction of the Sun's diameter.These prominences are among the longest-lasting solar phenomena with lifetimes of several days to weeks.The large field of view of AtLAST, combined with its good spatial resolution and the ability to observe the Sun on daily bases for extended periods, will offer us opportunities to study the questions of the prominence origin, evolution, and eventual instability.These are important questions, because the drivers that make the prominence magnetic field configurations unstable and erupt are still not well understood.Erupting prominences, as one of the main drivers of space weather, are then capable of hurling large amounts of magnetized plasma into interplanetary space at high speeds.However, it is unclear exactly what sets off these eruptions.
The simultaneous multi-band coverage, which is a capability that no other facility than AtLAST can provide with sufficient resolution, will allow us to answer also important questions about the thermal properties and energy balance of prominence plasma and to uncover the nature of the prominence plasma transition from cool cores to the hot corona.The advantage of observing at millimetre wavelengths lies in their easier interpretation (e.g.Heinzel et al., 2022;Labrosse et al., 2022).The spectral lines in the optical and UV used for prominence observations are typically optically thick so that detailed radiative transfer calculations are necessary for their analysis.In contrast, the prominence plasma is mostly optically thin at AtLAST wavelengths, which makes the interpretation much simpler due to relation between the observed flux and the plasma temperature of the emitting region (see, e.g., Gunár  Extremely valuable will be the joint observations of prominences with AtLAST and ALMA.ALMA interferometry is capable of very high spatial resolution, thus extending the observable domain towards the shortest resolvable scales.On the other hand, the interferometric (Fourier-based) observations are insensitive to the larger-scale structures (larger than the single antenna primary beam).In order to fill the gap around zero in the Fourier space, ALMA uses supplementary single-dish (SD) scanning when observing a multiscale structures, like prominences.However, the ALMA SDs have the same size of 12m and, consequently, there is a little overlap between the domains of scales covered by the high-resolution interferometric data and those obtained form the SD observations.With the much larger dish, AtLAST would provide an excellent bridge connecting both domains and allowing for a proper match of the interferometric and SD data.This is very true in general, but for the limb observations (prominences, spicules) even yet more vital.

The solar activity cycle
As stated above, millimetre observations have the advantage that the brightness temperatures corresponding to the observed continuum flux are thought to be a close proxy for the chromospheric plasma temperature with the formation height increasing with wavelength.Measuring the polarisation allows for deriving the line-of-sight component of the magnetic field.Daily full-disk maps of the Sun would permit the study of how the temperature (and hence the energy content) evolves in Active Regions, Quiet Sun regions and coronal holes.These data can be compared with other diagnostics, and in particular the evolution of magnetic fields in the solar atmosphere.The solar chromosphere is responsible for most of the UV emission that plays a major role in structuring the Earth's upper atmosphere, and evolution of the millimeter emission will in turn reflect the drivers of solar UV emission.As observations in different frequency bands probe different depths in the solar atmosphere, comparing the evolution in these different layers is important for understanding the transport of energy through the chromosphere.Repeated sets of such observations obtained over a period of years will reveal how the millimeter emission responds to the solar cycle.A noteworthy demonstration of the scientific potential is the sequence of observations with the Solar Submillimeter-wave Telescope (SST) that covers a period longer than one solar cycle (Menezes et al., 2021).
Measuring the solar radius at subterahertz frequencies (submm/ mm) allows one to probe the solar atmosphere, since these measurements show the height above the photosphere at which most of the emission at a determined observation frequency is generated (Menezes & Valio, 2017).Changes in the solar radius show it can be modulated with the 11-year activity cycle (mid-term variations) as well as longer periods (long-term variations).The equatorial radius time series was found to be positively correlated to the solar cycle, since the equatorial regions are more affected by the increase of active regions during solar maxima, making the solar atmosphere warmer in these regions; on the other hand, the anticorrelation between polar radius time series and the solar activity proxies could be explained by a possible increase of polar limb brightening during solar minima (Menezes et al., 2021).In the context of the study on the subterahertz solar atmosphere, spicules can affect the measurement of the solar radius and cause the solar limb to appear more diffuse, which can lead to an overestimation of the solar radius.In Menezes et al. (2022), the discrepancies between measured limb brightening values and model predictions highlight the need for further studies to improve our understanding of the solar atmosphere.Therefore, it is important to take into account the presence of spicules when measuring the solar radius and limb brightening at different frequencies.Currently, however, there are no full-disk observations of the Sun in the mm range apart from occasional ALMA TP maps a few times a year.
Please note that the Sun's rotation depends on latitude with a period of down to 24 days at the equator (see, e.g., Schou et al., 1998;Snodgrass, 1983).Any long-lived feature like an Active Region would thus move across the visible disk of the Sun in less than two weeks.However, at the resolution anticipated for AtLAST (see Figure 3), features like Active Regions and the sunspots (Solanki, 2003) therein would evolve significantly on a daily timescale.This use case would therefore be addressed best via full-disk mapping of the Sun at multiple frequency bands, once per day.Already an initial 1-month campaign covering a full solar rotation would allow for addressing the fundamental unsolved problems mentioned above including the nature of coronal and chromospheric heating problems and solar flares, whereas much longer sequences are required for addressing the solar activity cycle.
New insights regarding the Sun's activity variations and thus the long-term evolution of our host star could be transferred to other stars.This Sun-as-a-star approach has recently received increasing attention in the context of next-generation exoplanet observations for which it is crucial to separate observable exoplanet signatures from the host star's "background radiation".

The solar-stellar connection
The Sun, which can be observed spatially resolved, serves as a fundamental reference case for studying the dynamic nature of stellar atmospheres and solar/stellar activity including the occurrence of flares (see Section 2.  on timescales of a few seconds to minutes.Observing the temporal evolution of a flare, which is essential for exploring the physical mechanisms, thus requires time sequences with accordingly high temporal cadence.Such data sets are typically not generated from a serendipitous detection or as part of a survey but require a dedicated sit-and-stare observation of the same region in the sky. AtLAST would be capable of such sit-and-stare observations, providing crucial time-resolved light curves for stellar flares.Given the high sensitivity of AtLAST, stellar flares in cool main sequence stars at distance of up to ∼50 pc should be detectable with integration times of a few seconds, thus resolving the relevant timescales.In addition, the anticipated unique capability of observing at multiple frequencies simultaneously, which is typically not provided by other sub-mm instruments and surveys, especially when combined with polarisation capabilities, would enable AtLAST to utilise essential diagnostics such as the variation of the mm spectral index, an indicator of stellar atmospheric activity (Mohan et al., 2022), and strong constraints to the emission mechanism and estimates of the magnetic field strengths in the flaring active regions.
The full potential of flare observations at millimeter wavelengths is only unlocked through coordinated, strictly cosimultaneous observations with other telescopes covering as large a wavelength range across the electromagnetic spectrum as possible.Such coordinated campaigns, which have become common in multi-messenger astronomy and are basically standard procedure for observations of the Sun, demand for PI-driven operations.The scarcity of such coordinated stellar observing campaigns is among the main reasons why there is still no confident detection of a stellar coronal mass ejection (CME) -an essential component of exo-space weather.The success of such campaigns would be greatly enhanced by AtLAST's large FOV and high angular resolution, thus being able to observe multiple stellar targets at the same time while separating the flare source(s) from other components such as close-by active companion stars or disks, making AtLAST ideal for time-resolved coordinated observations of stellar flares.See also the time-domain science cases for AtLAST (Orlowski-Scherer et al., 2024).

Diagnostic capabilities and instrumental requirements
There are two major constraints for solar observations at millimeter wavelengths: (i) As the Sun is by far the brightest millimeter source in the sky, sensitivity is not an issue and very short integration times and thus even on-the-fly scanning is possible.(ii) The Sun evolves on short time scales which prohibits long integration/scan times.Imaging of solar data thus needs to be done as snapshot imaging or over short time windows that should not exceed 1 min for the expected resolution (on the Sun, temporal and spatial scales tend to correlate).As will be detailed in this section, the combination of high angular resolution, high temporal cadence (or at least short integration time), wide frequency coverage, and large dynamic range are crucial for meaningful solar observations with AtLAST (Mroczkowski et al., 2024).In addition, full-Stokes polarimetry would greatly enhance AtLAST diagnostic potential for the Sun.

High angular resolution and spatial mapping.
High spatial resolution is of utmost importance for solar observations as much of the relevant dynamics occurs on small spatial scales.Achieving sufficiently high resolution is challenging at millimeter wavelengths, in particular for single-dish telescopes such as AtLAST.While AtLAST's aperture sets a limit, the achievable resolution is still in the relevant range and superior to any previous single-dish observation of the Sun.With an aperture of 50 m, the achievable angular resolution would be 6.5" at a wavelength of 1.3 mm (ALMA Band 6) and down to just 1.5" at 0.3 mm (ALMA Band 10) (see Figure 4).The roughly 4 times larger aperture of AtLAST compared to an ALMA 12-m antenna results in an accordingly much smaller (∼6 %) beam area.Scanning the whole disk of the Sun would take considerably longer, which would be sufficient for synoptic studies with just one scan per day but prohibitive for science cases that rely on high temporal cadence.In the latter case, scans would then need to be limited to smaller region, although a compromise between size of the mapped region and overall cadence can be made.In either case, for a time series, the scanning could be continuous.
A multi-pixel detector would significantly enhance the diagnostic possibilities for solar observations with AtLAST.Even for a modest setup with a detector with 1000 pixels in a concentric setup with no overlap, spaced by one beam width, the resulting instantaneously covered region on the Sun (hereafter referred to as the instantaneous field of view, FOV) would cover a region with a radius of about 36 beams.While a single AtLAST beam would be a factor 50/12 smaller than the beam of a 12 m ALMA antenna, using 1000 pixels would effectively make the instantaneous 12 FOV 36 9 50 × ≈ times larger.As shown in Figure 4, the diameter of the FOV would range from ∼ 45" at 950 GHz (ALMA Band 10) to ∼ 450" at 100 GHz (ALMA Band 3).Such a FOV would cover a complete sunspot even at the highest frequencies and whole Active Regions at the lower frequencies (see Figure 3).The angular resolution of the final imaging products could be increased by means of a rapid small scan pattern (on scales comparable to the beam size and below) that compensates for the above described pixel spacing.The diameter of the instantaneous FOV would be halved again for a denser pixel setup that allows for Nyquist sampling, which then would not require the mentioned scan pattern.Please see Section 3.3 for a detailed discussion of the detector requirements for solar observations.Multi-frequency synthesis might offer means to further increase AtLAST angular resolution.However, as the formation height range of the mm continuum depends on the frequency, only a moderate frequency range should be considered.Depending on the receiver design, multi-frequency synthesis could be an option that could be applied flexibly on AtLAST data sets.

Frequency coverage and spectral setup.
An essential aspect to the continuum radiation is that the formation height range from where most of the emission emerges depends on the observing frequency or wavelength.At the highest frequency accessible with ALMA, i.e. 950 GHz (or a wavelength of 0.3 mm), the continuum radiation stems from the upper photosphere and lower chromosphere, whereas the continuum radiation at the shortest frequency of 35 GHz (equivalent to a wavelength just short of 1 cm) originates from the uppermost chromosphere with possible contributions from the transition region.Covering a large frequency range simultaneously or at least rapidly scanning through frequency has thus the potential to map a large height range in the solar atmosphere.In case of scanning through frequency, the scanning speed must be short compared to the dynamical timescales in the solar atmosphere, which are down to seconds and generally well below 1 min (depending also on the achieved spatial resolution).
Observations that cover extended regions on the Sun (or even the whole Sun) across a large frequency range would enable the reconstruction of the three-dimensional thermal structure of the solar chromosphere via tomographic and inversion techniques.Producing a time series at sufficiently high cadence would then enable to assess the temporal variation of the 3D structure -a data product with the potential of truly ground-breaking scientific impact for a very large range of essential topics in solar physics.
The observable frequency range should extend at least from 90 GHz to 660 GHz.Observing at higher frequencies of up to 1 THz would provide higher angular resolution but adequate observing conditions may not occur every day, making these bands unreliable in the context of daily synoptic observations.Even for continuum observations, a high frequency resolution is desirable but already a frequency increment of ∼ 100 GHz would allow for excellent scientific results.
While the aforementioned considerations apply to continuum observations, a large number of spectral channels with high spectral resolution and a flexible set-up of the receiver bands would offer additional possibilities.While it has yet to be seen if spectral lines, mostly hydrogen recombination lines and potentially CO, can be detected at millimeter wavelengths, they would have large diagnostic potential for assessing the thermal, kinetic and magnetic state of the chromospheric plasma.It is difficult to answer right now which frequency setup would be necessary to exploit the diagnostic potential of spectral lines but, based on tentative simulations, hydrogen recombination lines might be spread out over one or a few GHz but would require nonetheless a spectral resolution better than 15.6 MHz (as currently offered by ALMA) in order to exploit the full diagnostic potential (e.g., Doppler shifts for line-of-sight velocities).

Sensitivity, integration time, dynamic range.
The Sun is by far the brightest millimeter source in the sky with typical brightness temperatures of several thousand Kelvin.Consequently, sensitivity is not a concern and the integration time can be very low, allowing for ultra-high cadence, which is of essence for a range of science cases.The integration time can be much below 1 s depending on possible attenuation strategies (e.g., solar filter or detuning).Important for solar observations, however, is a large dynamic range.ALMA observations in Band 3 and 6 show a wide range of brightness temperatures from as low as 3000 K to above 13 000 K (see, e.g., data sets in the Solar ALMA Science Archive, Henriques et al., 2022).In general, mean brightness temperature of the Sun depends on the frequency because the atmospheric height range of the mapped layer depends on frequency and thus on the thermal stratification of the solar atmosphere.In principle, the highest ALMA receiver bands map the transition between the upper photosphere and lower chromosphere (i.e., the classical "temperature minimum" region) with comparatively low temperatures, whereas the lowest ALMA bands map radiation emerging from the on average much hotter upper chromosphere close to the transition region with its steep jump in temperature.However, as mentioned in Section 2.2, solar flares are a key science case for solar observations with AtLAST.Depending on the strength (i.e.overall energy release) of a flare, plasma temperatures exceed 10 6 K or even 10 7 K.A flare thus emits orders of magnitude more radiation than the average (quiescent) Sun as discussed above.It should be noted that the corresponding peak brightness temperature also depends on the observing frequency and the beam size, which is typically too large to resolve the source.From observations of a (very strong) X-class flare with the 1.5m-aperture Solar Submillimeter Telescope (SST, Kaufmann et al., 2008) at 212 GHz an excess brightness temperature of 1.75 × 10 6 K for an assumed source size of 25", which would remain unresolved (Giménez de Castro et al., 2018).In comparison, AtLAST would have an angular resolution of ∼7" at 212 GHz and would thus be able to resolve the source and thus brightness temperatures in excess of 10 6 K.At shorter wavelengths in the sub-mm range, we rely on simulations to estimate the expected brightness of flares (see Figure 2).
Addressing the full range of science cases would thus require to account for a brightness temperature range from typically 3000 K up to 14 000 K for the non-flaring Sun, depending on frequency and resolution, but up to millions of K for flares.
Consequently, obtaining a large dynamic range for solar observations and at the same a high sensitivity for non-solar observations is a big challenge for designing of a receiver system that is intended to cover all science cases.

Polarisation.
Magnetic fields play an essential role in the Sun's structure, dynamics, and activity.Their impact is clearly visible in Active Regions most notably in the form of sunspots and as large-scale prominences but also the Sun's Quiet Regions harbour magnetic fields in various configurations and strengths.The latter becomes immediately obvious from high-resolution Hα observations (see, e.g., Rouppe van der Voort et al., 2023;Rutten et al., 2008).High-resolution magnetograms obtained from the spectral lines in the photosphere (i.e., the Sun's surface layer) have become a staple in contemporary solar physics relevant to a large range of scientific topics but often also just for context.Reliably measuring the magnetic field in the solar chromosphere above, i.e. the layer that would be observed with AtLAST, is still a current technological challenge, again with much diagnostic potential.The measured polarization state provides a measure for the longitudinal component of the magnetic field vector in the same layer as the continuum radiation.In the same way, a scan through wavelength (and thus through formation height) can be used to reconstruct the three-dimensional magnetic field structure in the solar chromosphere.Measuring the magnetic field in this layer is in itself a hot topic with potentially ground-breaking results.
Early observations with ALMA at a frequency of 100 GHz, which were obtained as science verification data in Band 3 (ADS/JAO.ALMA#2011.0.00011.E), indicate that the circular polarization degree is at least 1%.This value is considered a minimum, as the observations were carried out with the 12m-Array only (Shimojo et al., 2024).First regular ALMA observations of the Sun with full polarisation in Band 3 are scheduled for Cycle 10.Important lessons are expected from these observations, which would have implications for full polarisation observations with AtLAST.In general, circular polarization levels of up to 5% are expected for the Sun at mm wavelengths.

Observing modes
In order to address the aforementioned key science cases (see Section 2), it would be best to combine 1) long-term synoptic observations with a very low daily load on observing time with 2) campaign-based observations.The synoptic observations could consist of one daily full-disk map or preferably a 10 min long time sequence of maps across a wide predefined frequency range.The resulting long-term data set would be of essential value for studying the solar cycle and all related variations imprinted in the Sun's chromosphere with fundamental implications for stellar activity cycles and their impact on the habitability of exoplanets (White et al., 2023).The campaign-based observations would be more adjusted towards the requirements of individual science cases.The scheduling for observations that require the existence of an Active Region could be planned with just a few days ahead as the co-ordination with other space-borne and ground-based observatories would boost the scientific impact of such AtLAST data.Alternatively, a ToO mode (also possibly confined to a campaign) would ensure to observe flares whenever a suitable Active Region appears.

Solar observing mode 1 -Synoptic full-disk scans.
A field-of-view (FOV) that would cover the whole Sun plus a margin around, which is important to include the Sun's outer atmosphere, has a diameter of ∼ 2000".Scanning such a region with the comparatively small beam size of AtLAST would require long scan times.Therefore we expect that multi-pixel detectors will be needed for solar disk mapping as well as other non-solar large FOV studies.The corresponding time needed for scanning the whole FOV would be reduced basically by the number of simultaneously used beams (pixels) and thus the resulting size of the instantaneously covered FOV (see also Section 3.1.1).The required scan time for the whole solar disk would scale accordingly with respect to the single-dish Total Power scans with ALMA antennas, which take about ∼ 10 min.Consequently, a full-disk scan at the lower frequencies could potentially be completed in a few minutes or less, aided by the anticipated high slew speed of 3 deg/s.A smaller number of pixels, e.g.∼ 250 pixels, would directly affect the covered FOV, resulting in correspondingly longer scan times.Please note that very short integration times are sufficient as the Sun is the brightest mm source on the sky, and correspondingly mapping speed is not at all dependent on sensitivity requirements, rather it depends solely on the receiver FOV and antenna slew rates.See Section 3.3 for more considerations regarding multi-pixel detectors.
The short times for completing a scan of the whole solar disk would allow for scheduling a daily solar map, which would have enormous potential for studying the long-term evolution and the solar activity cycle (see Section 2.4).

Solar observing mode 2 -High-resolution time-dependent observations.
A selected target, e.g. a sunspot (see Figure 3), would be followed in time for one or several hours (compensating for motion on the sky plus solar rotation) and observed with preferably high cadence.For comparison, ALMA currently observes the Sun at 1 s cadence.This mode, which is equivalent to observations at visible wavelengths at limited field of view, is suitable for a large range of science cases that require a combination of high spatial and temporal resolution.

Solar observing mode 3 -Regional scan sequences.
As a compromise between full-disk scans (mode 1) and single-target tracking (mode 2), AtLAST could perform scans of extended regions (or mosaics).The size of the covered region on the Sun would depend on the instantaneous field of view of the multi-pixel detector (see Section 3.3) and the maximum acceptable temporal cadence.Such scans could be repeated continously for some time, e.g. one hour, providing good temporal cadence of a large field of view.This mode could be useful for observations of large-scale features such as filaments or entire Active Regions.Such observations would facilitate the detection of flares and filament eruptions and at the same time capture their evolution at adequate temporal resolution.

Instrumentation
The detectors described in this section assume technological progress on a time scale of about 10 years.The specifications are provided by the AtLAST instrument working group (https://www.atlast.uio.no/memo-series/memo-public/instru-mentationwgmemo4_29feb2024.pdf).Please note the proposed instruments would have different operation modes and would also be suited for slightly different science cases.In Figure 4, the instantaneously covered FOV of multi-pixel detectors with n pixels are illustrated.The pixels are assumed to the same diameter as the beam diameter d beam at a given observing frequency and are packed with no overlap.Treated as a circle packing problem, the resulting diameter of the FOV is approximated as fov beam 2 3 3 / .

Multi-chroic continuum camera.
A first-generation multi-chroic camera for continuum observations could have 30 000 pixels covering 3 frequencies simultaneously while a second-generation camera could be extended to possibly 300 000 pixels covering 6 frequencies simultaneously.The frequencies would be preferably spread equally over the range from ∼ 100 GHz to 700 GHz but adjusted according the atmospheric transmission at the AtLAST site, e.g., 100, 220, 340, 460, 615, and 700 GHz (see https://almascience. eso.org/about-alma/alma-site).Full polarisation capability would substantially enhance the diagnostic possibilities (see Section 3.1.4).
The details of the detector setup have to be investigated in detail.That includes the spacing between pixels, the total number of pixels, and the resulting instantaneously covered FOV.A fast small circular scanning pattern could be used to fill intermediate pointings.Combining data from circular scans (if possible on a second time scale or at least <10 s) would then allow to produce data with higher angular resolution.A detailed study is currently in preparation (Kirkaune et al. in prep.).

Multi-pixel heterodyne receiver system.
A full heterodyne system with 64 spectral pixels (spaxels) and 16 GHz bandwidth seems technologically feasible, whereas, on a 10-years perspective, systems with at least 256 spectral pixels (spaxels) and 30 GHz bandwidth might become possible.Such a detector would allow for exploiting the spectral domain but comes at the price of a much smaller number of detector elements as compared to multi-chroic continuum cameras (see Section 3.3.1),strongly limiting the instantaneously covered region on the Sun.In combination with spatial scanning strategies, multi-pixel heterodyne receiver system would require compromises between covered field of view and overal temporal cadence, which would be needed to adjusted to the needs of individual science cases.These limitations would only make sense if spectral lines are discovered on the Sun that would justify these limitations for accessing the diagnostic potential of spectral lines (see Section 3.1.2).

Integrated Field Unit.
While multi-chroic continuum cameras (see Section 3.3.1)and heterodyne receiver systems (see Section 3.3.2) are the extreme cases considered here in terms of field of view versus spectral resolution, Integrated Field Unit could provide a compromise.First generation units are expected to have a spectral resolving power of R = λ/dλ = 500 with 10 000 detectors (number of spaxels × number of channels) and a frequency range of 70-690 GHz, second generation units could reach R = 2000 with 50 000 detectors covering an even wider frequency range.While a resolving power of R = 2000 would open diagnostic possibilities for spectral line observations in a narrow frequency range, it would only make sense if spectral lines at mm wavelengths are observable in the Sun at all.Integrated Field Units would be less efficient than multi-chroic continuum cameras for observing a large frequency range and thus a large height range in the solar atmosphere due to the still limited number of spaxels.With even only 10 frequencies, only 5000 spatial pixels would be available, which is considerably lower than what is expected for multi-chroic cameras.As for multi-pixel heterodyne receiver systems, IFUs would likely only make sense if spectral lines can be observationally exploited.In any case, a realistic evaluation of the scientific potential of IFUs will require a dedicated study.

Synergies for development and co-observing
Given the complex and dynamic nature of the solar atmosphere, coordinated multi-wavelength multi-instrument observing campaigns are the default modus operandi.This typically involves ground-based and space-borne observatories, which provide complementary data exploiting different continua and spectral lines across the whole spectrum, thus providing large data sets that probe the (ideally complete) thermodynamic and magnetic state of the solar plasma across preferably all atmospheric layers.While such coordinated campaigns are subject to the different time zones of participating instruments, there are many successful examples including ALMA observations of the Sun, which are typically complemented with space-borne observations with the Solar Dynamics Observatory (SDO) and the Interface Region Imaging Spectrograph (IRIS).

Summary of telescope requirements
AtLAST (Mroczkowski et al., 2024) observations of the Sun would produce a large range of valuable contributions to science cases that are difficult if not impossible to address with other existing or planned observatories.The need of high temporal, spatial, and to some extent spectral resolution makes adequate solar observations challenging.At the same time, resolution in one dimension can be sacrificed to boost the resolution in another dimension, e.g., lowering the temporal cadence for increased spatial resolution.Consequently, the best approach combines a multi-pixel detector with fast on-the-fly scanning.Appropriate imaging strategies could be developed during the commissioning phase and through simulations at an earlier stage.Additionally, in case that spectral lines at mm wavelengths are discovered in the Sun, heterodyne receiver systems of IFUs might have important scientific applications but require dedicated studies to realistically assess the feasibility and applicability given the limited possible detector sizes.Since the Sun is a very bright mm source, it could even be possible to split the optical path and feed multiple instruments that are optimised for different, complementary diagnostic purposes.Also, it has yet to be seen which solar science cases require instruments specifically designed for solar observing and which cases could be addressed with general instruments.
To fully unlock AtLAST's potential in this respect, the following instrumental properties are essential: • Sufficient instantaneous field-of-view: A multi-pixel detector is a fundamental requirement as the instantaneously covered region on the sky with a single beam would be insufficient for most solar science cases.
• Wide frequency coverage: A wide (quasi-)simultaneous frequency coverage beyond the current setup of ALMA's receiver bands, possibly even covering the whole frequency range from (at least) 90 GHz to 660 GHz, has large scientific potential as it facilitates simultaneous mapping of an extended height range in the solar atmosphere.A multi-chroic camera with a large number of pixels seems to be a promising choice for continuum observations.
• Full polarisation capabilities are desirable in order to provide information on chromospheric magnetic fields.
• High temporal cadence: While integration times are very short for a bright object like the Sun, spatial (or spectral) scanning in order to cover an adequate spatial (or spectral) region is constrained by the short dynamic timescales.Preferably, the temporal cadence should be less than 1 min but the shorter the better.High detector readout rates are required, especially for fast scanning.

• Adequate brightness temperature range and accuracy:
As the Sun is the brightest mm source in the sky and can vary in brightness significantly, in particular during flares, a solar filter with well-defined characteristics and large dynamic range for the detector are needed.
A brightness temperature accuracy of 100 K or better is important for solar science cases.Consequently, the need for detector cooling will depend on the achievable signal-to-noise ratio.
• Spectral resolution: Spectral lines -if successfully detected in the Sun -would enormously increase the diagnostic capabilities.Designing a suitable instrument, possibly based on Integrated Field Units, would require a dedicated study.

Open Peer Review
Current Peer Review Status:

Malcolm Druett
The University of Sheffield Department of Automatic Control and Systems Engineering, Sheffield, England, UK

Review Summary
I was very pleased to read this paper, as I consider the instrument under to discussion to be a very exciting addition to the fleet of instruments we can use to study the Sun and other stars.This paper highlights several promises to advance our understanding of many active research themes using the instrument: coronal heating, the nature of prominences, the production of CMEs and long-term activity cycles.Moreover, this instrument has the potential to add to the joining up of science with millimeter wavelength range co-observations, as well as strengthening our understanding of the links, differences, and gradients in behaviours between our Sun and other stars.
One point I would appreciate the authors addressing is that I was expecting to be first presented with clear, concise summary of the proposed observational parameters before the science use cases in order to be able to understand and evaluate these.The ordering of the sections is such that if you are unfamiliar with the instrument, as many readers may be, you must simply accept the claims about the suitability for each science use case when reading through the paper in order.This concern could be addressed through clear referencing to specific points in later sections, a summary table, or restructuring of the paper.
Also in some of the sections where science use cases are presented, I recommend stronger links to be drawn between the observational capabilities of this instrument and the constraints required to address those science questions.Without these links made explicit to the reader I believe that the current version of the manuscript has sections that are diluted in informational value, with un-cited, uncorroborated, or decontextualised claims.
The author list boasts an exceptional array of talent that I am certain is capable of addressing these concerns.I recommend edits are made before acceptance.

Introduction
(1) "The thermal and magnetic structure of the chromosphere is complex and highly dynamic with a plethora of physical processes at work, many of which induce notable deviations from equilibrium conditions (for example in the ionisation state of hydrogen).The largest features like filaments can span substantial fractions of the solar diameter ( 30')" This phrasing suggest filaments to be chromospheric plasma rather than cool dense coronal plasma.I recommend the authors to re-phrase this.
( (3) The following point is relating to the discussion in this section, I would like to hear the author's feedback on this, but it is not necessarily something that needs to be included in the text unless there are elements that the authors would deem worthwhile enough for inclusion, for example to bolster the strength of claims made within the later sections.
Many of the current authors were also involved in the publications of

Key Science Cases
(5) "The chromosphere is an integral part of the solar atmosphere and as such plays an important role in the transport of energy and matter.These are essential for understanding the heating of the corona, the origins of the solar wind, and the drivers of solar activity and space weather.There is a plethora of physical processes involved, which are entangled in complicated dynamic ways, rendering the understanding of the workings of our Sun a challenging undertaking." (a) citations needed.(b) "The chromosphere is an integral part of the solar atmosphere and as such plays an important role in the transport of energy and matter."This sentence currently has low informational value.I suggest either -simply stating that the chromosphere plays an important role in the transport of energy and matter with some citations or -actually explaining what you mean by a little in terms of it being "an integral part" of the solar atmosphere and why.For example, one could argue this in terms of the behaviour changes either side of the plasma beta=1 layer, wave propagation, and non-equilibrium conditions.I am not a fan of characterising something as complicated or shrouded in mystery for the reader to understand that there are unresolved, interesting, and valuable science questions.It would be great if the authors could add some detail to pull back the curtain of mystery and complexity a little.( 6) "As detailed in the sections below, AtLAST (Mroczkowski et al., 2024) opens up a new window to science cases that cannot be addressed with existing sub-mm telescopes.In addition, some solar science cases for ALMA (see Bastian et al., 2018; Wedemeyer et al., 2016, and references therein; see also Figure 1) and LLAMA (Lépine et al., 2021) are potential solar use cases for AtLAST, too, thus creating synergies between these observatories.These science cases concern the thermal structure of the solar atmosphere including the thermal structure of prominences and filaments, the related transport of energy and mass, and phenomena related to solar activity.In the following, the key science cases for AtLAST are highlighted."(a) I do not see the authors linking Figure 1 to anything stated above.The images show two time points in the solar cycle.To clarify, I am certain that solar cycle data from ALMA has valuable information.However, since none is mentioned or explained here, figure 1 appears to be only a visually satisfying image.Please provide some context in the caption or the text.This could even be a reference to the later point in the paper where this figure is discussed.
(b) Are you saying these listed science cases will be addressed in the following sections?If so, then I request you say that.If not then the statement is too brief to provide any information of value to the reader and I recommend adding citations, context, or both.
2.1 Thermal structure and the atmospheric heating problem (7) The first part of this section is very nicely stated, although again lacking any citations beyond one early paper relating to the coronal heating problem.Please add citations.
"In principle, identifying these mechanisms and understanding their contributions requires quantitative and precise measurements that capture the thermal, magnetic, and kinetic state of chromospheric plasma over time and in three spatial dimensions.AtLAST has the potential to provide such data."At this point in the paper, the reader has not been provided with an overview of the capabilities of the instrument, nor have you provided citations with reasoned explanations or estimated of what observational capabilities could be required to derive these properties at the cadences and spectral/spatial resolutions required.Thus, unless the reader is already previously aware of all these details they have to accept the claim on trust.As stated in the summary I recommend this concern could be adequately addressed with context, references to later sections, or restructuring of the paper.

Solar Flares
(8) "AtLAST is poised to make significant contributions in addressing numerous unresolved inquiries pertaining to solar flares, a prominent conundrum within contemporary solar physics that continues to be a highly dynamic area of investigation.Although numerous intricacies remain shrouded in mystery, it is evident that solar flares manifest as a result of the dynamic reconfiguration and interconnection of magnetic fields within the solar atmosphere."Citations needed here.But I thank the authors of this section for providing sufficient citations elsewhere.
(9) "And yet, it cannot be ruled out that even stronger flares exceeding the Carrington event of 1859 could occur with disastrous consequences for our technology-dependent modern society.Such so-called super-flares are observed for other (solar-like) stars (Maehara et al., 2012) (see Section 2.5).The study of strong solar flares, to which AtLAST can contribute in new ways, is thus of utmost importance."At this point in the paper without any solid evidence provided of how AtLAST can contribute, we are taking this "utmost importance" on faith.I recommend the authors to talk about the ways in which it can contribute explicitly.For example describing the observational capabilities, cadences, resolutions, atmospheric parameters, and how these relate to the flare science questions identified.
(10) Figure 2: I assume the close association of mm-continuum radiation with brightness temperature will providing information to answer particular science questions.The relationship in flares is nicely demonstrated by the figure.Please point this out, and mention some of the science cases this will address and explain how the information will help.(11) "Observations of such sub-mm flares might also provide key information about the formation of hot onsets in solar flares (da Silva et al., 2023;Hudson et al., 2021)."What sort of key information?Why "might"?Can you analyse whether the information obtained would help address the science questions?I recommend talking a bit about the science questions, the observational requirements and how AtLAST can provide observations that meet those requirements.
(12) "Addressing these aspects with AtLAST would require high spectral, spatial and temporal resolution and preferably full polarisation" And can/do we have that?The observational capabilities of the instrumentation have not been summarised or discussed.Please address whether you believe this is feasible and justify your position to the reader.

Solar Prominences
(13) "These prominences are among the longest-lasting solar phenomena with lifetimes of several days to weeks.The large field of view of AtLAST, combined with its good spatial resolution and the ability to observe the Sun on daily bases for extended periods, will offer us opportunities to study the questions of the prominence origin, evolution, and eventual instability." The paragraph below this one makes a nice case for mm studies of prominences.
I recommend that the discussion could be supplemented in several ways: (a) citations where appropriate.(b) are there physical processes relating to prominence formation/evolution/instability that occur at scales and cadences you anticipate to be evident at AtLAST's resolution (please also state that resolution), which are not currently accessible via existing solar mm instrumentation?(c) it may also be worth mentioning the validation and calibration you could perform on estimates of plasma quantities that are otherwise made using inferences from complicated optically thick radiative transfer.( 14) "because the drivers that make the prominence magnetic field configurations unstable and erupt are still not well understood."& "However, it is unclear exactly what sets off these eruptions."Repetition

Solar Activity Cycle
(15) I recommend that this section could do with a few more citations for the results you discussif possible not so dominantly from one of your authors, Menezes.Also please define TP in the text.( 16) "Please note that the Sun's rotation depends on latitude with a period of down to 24 days at the equator (see, e.g., Schou et al., 1998;Snodgrass, 1983).Any long-lived feature like an Active Region would thus move across the visible disk of the Sun in less than two weeks.However, at the resolution anticipated for AtLAST (see Figure 3), features like Active Regions and the sunspots (Solanki, 2003) therein would evolve significantly on a daily timescale.This use case would therefore be addressed best via full-disk mapping of the Sun at multiple frequency bands, once per day."Please clarify which use case you are referring to -Are you talking about studying the solar cycle in general or some specific observational case within that?
(17) "New insights regarding the Sun's activity variations and thus the long-term evolution of our host star could be transferred to other stars.This Sun-as-a-star approach has recently received increasing attention in the context of next-generation exoplanet observations for which it is crucial to separate observable exoplanet signatures from the host star's "background radiation"."Citations needed.
The Solar Stellar Connection (18) This section does several things very well that should be highlighted for interpreting my other comments in this review.(a) cites papers when claims regarding physical processes are made that relate to the science cases.
(b) relates stated capabilities and resolutions/cadences of the instrument directly to the use cases under discussion.
The spectrum of cited authors and findings within the field is rather limited, I suggest a more comprehensive coverage, but other than this the I have no notes on the section.
3 Observing the Sun with AtLAST (19) The information in this section would have been useful to know earlier, or at least be referenced from the earlier sections.Also given some of the abbreviations are defined in section 3 and used in section 2 I would assume there was already some debate regarding this ordering.Please make section 2 easier to follow for first time readers by linking the claims to information from section 3.
(20) "The Sun evolves on short time scales which prohibits long integration/scan times."I recommend changing the word "prohibits" to another word, as this doesn't really prohibit long integration times, it just devalues them for resolving transient structures.
(21) "While it has yet to be seen if spectral lines, mostly hydrogen recombination lines and potentially CO, can be detected at millimeter wavelengths, they would have large diagnostic potential for assessing the thermal, kinetic and magnetic state of the chromospheric plasma."Could you comment on whether there is any ongoing effort to look into the existence of these lines within the proposed spectrum?Do you intend to conduct such a search in the early use cases?

Sensitivity, Integration time, Dynamic range
(22) Regarding the points made in the final paragraph, please could you comment on the outlook for being able to cover the necessary for studying flares?Perhaps some mention of this would be useful in the text too.I do believe there would be very useful information to glean about flare ribbons, condensation and evaporation even from a more limited dynamic range.

Polarisation
(23) "magnetograms obtained from the spectral lines in the photosphere (i.e., the Sun's surface layer)" This is the 4th instance of the word photosphere.If you wish to explain what it is, I would recommend doing so at the first instance.
(24) "Reliably measuring the magnetic field in the solar chromosphere above, i.e. the layer that would be observed with AtLAST, is still a current technological challenge, again with much diagnostic potential."Citations to works from Pietrow, Morosin, and Vissers plus any the authors wish would be useful here [ .
(25) "Early observations with ALMA at a frequency of 100 GHz, which were obtained as science verification data in Band 3 (ADS/JAO.ALMA#2011.0.00011.E)," I recommend considering if this is the best way to cite this data.Perhaps providing a footnote or a reference to its description elsewhere in the document that says what this is and how to obtain it.

Observing modes 3.2.1
(26) "with respect to the single-dish Total Power scans with ALMA antennas" TP is now unabbreviated.I agree with the final statement of this section, that would be a most welcome addition to our field.

Instrumentation
(27) "the resulting diameter of the FOV is approximated as d fov ≈ ..." For clarity, I recommend using a format that makes it explicitly clear what is, and what is not, under the large square root.This could also be achieved satisfactorily with parentheses.

3.3.1
(28) "The details of the detector setup have to be investigated in detail.That includes the spacing between pixels, the total number of pixels, and the resulting instantaneously covered FOV.A fast small circular scanning pattern could be used to fill intermediate pointings.

Alexander G.M. Pietrow
Leibniz Institute for Astrophysics Potsdam, Potsdam, Germany This manuscript discusses the construction and utilization of the 50-meter single-dish Atacama Large Aperture Submillimeter Telescope (AtLAST).The primary goal is to provide a comprehensive sub-mm diagnostic tool for studying the Sun's chromosphere, and that of other stars.This telescope will help fill the resolution gap around zero in Fourier space, and its large size will allow for overlap between the ALMA resolution space in a way that the existing 12-meter single dishes cannot.This is a timely and valuable project that will help further explore solar and stellar spectra beyond the infrared.However, several aspects of the current version of the paper are unclear.Therefore, I suggest making modifications to address these issues before the paper is accepted for indexing.Additionally, some minor points could be improved in the revised manuscript

4.
Page 7, second column, second paragraph; I believe that the word associated should be correlated instead.

5.
Page 7, figure 2; Please mark the AtLAST bands on the figure, or mention them in the caption.

6.
Page 8, section 2.3; Perhaps a link could be made with prominence models and how measurements in the sub-mm would provide valuable constraints for such models (e.g.[ ).

7.
Page 9, first column, first paragraph; The acronym TP has not been defined.8.
Page 9, first column, second paragraph; It is not fully clear if this paragraph suggests a high-cadence observing mode, or daily full disk images.I believe that it is the latter, but in that case, solar flares should be removed from this list as the odds of capturing them are very low for daily maps.Unless the authors mean that tracking the evolution of active regions will shed light on flare physics, in which case this should be clarified.Additionally, the Solanki reference should be moved to the first mention of sunspots and perhaps  could be added where it is pointed out that active regions move at different velocities than the quiet Sun.

9.
Page 9, second column, second paragraph; I believe that a bigger summary should be given concerning sun-as-a-star observations in other wavelengths and how AtLAST would add to these programs.Some suggested citations on instruments, and Sun-as-a-star work done with these instruments concerning Sun-as-a-star flares can be found in [Ref 14 -19].A short discussion of how resolved vs unresolved flare studies [Ref 17 -19] help with 10.
understanding flare observations would fit here.Additionally, if a flare is caught at a high cadence with a limited FOV, would it be feasible to turn this into a sun-as-a-star observation using a method similar to e.g.?Page 9, figure 3; Please add an additional panel that shows the resolution with an ALMA SD dish.This would give a good comparison between existing and proposed instrumentation.

11.
Page 10, first column one, third paragraph; "...still no confident detection of a stellar coronal mass ejection…" This is a very strong statement that would need to discuss proposed detections and explain why they are not confident.I suggest saying that only a relatively low number of CMEs has been detected so far, and cite [ . 12.
Page 10, first column one, fourth paragraph; "...very short integration times and…" Could you give an order of magnitude value here?13.
Page 10, second column one, second paragraph; The last part of this paragraph should be moved to the front (See point 2).

14.
Page 10, second column one, second paragraph; "On-the-fly scanning" How is this different from taking a mosaic?If it is not, perhaps it could be mentioned that this is similar or equivalent to taking a mosaic.In section 3.2.3(pp13) they are equated to mosaics.

15.
Page 11, figure 4; Please add a wavelength axis to panels a and b, as was done in Fig. 2. Additionally, should the vertical solid line in panel b also be dashed?

16.
Page 12, first column, second paragraph; The cited source does not discuss cold temperatures below ~4500 K, perhaps the authors could add a small discussion on these lower temperatures and their implications, given that they are below that of the temperature minimum.Citation 4 (last part of section 4.1) offers a good summary and an explanation of why other chromospheric proxies are not sensitive to these temperatures.Page 13, first column, second paragraph; "..would require long scan times."Please give an order of magnitude estimate.The latter part of this paragraph does explain it somewhat, but I suggest this is edited to be more clear.

23.
Page 13, second column, second paragraph; equation on the last line.Please give in larger mode for readability and give a numerical approximation of the constant.

24.
Throughout; The manuscript has a preference for frequency over wavelength when discussing bands, however, it gives both at some locations in the text.I suggest that this is homogenized and that the wavelength is also given to improve readability for those outside of radio astronomy.Reviewer Expertise: Solar physics, Sun-as-a-star observations, flares, and spectropolarimetric inversions.
I confirm that I have read this submission and believe that I have an appropriate level of expertise to confirm that it is of an acceptable scientific standard, however I have significant reservations, as outlined above.
2.1) in a more continuous way across most of the Sun, whereas strong flares are associated with Active Regions.Despite many decades of research and significant progress, there are still many open questions regarding central aspects of solar and stellar flares on all scales including the particle acceleration mechanisms (e.g.Miller, 1998), quasi-periodic pulsations (e.g.Mohan, 2021; Simões et al., 2015), and the source of the still enigmatic emission at sub-THz frequencies (Fleishman & Kontar, 2010; Kaufmann et al., 1985; Kaufmann et al., 2004; Krucker et al., 2013), i.e. in the frequency range to be covered by AtLAST.Observations of flare-like brightenings with ALMA, in both interferometric mode (Rodger et al., 2019; Shimojo et al., 2017a) and single-dish (Skokić et al., 2023), have revealed faint and localized sources, likely thermal in origin, and well associated with the observed emissions in EUV and SXR.Observations of such sub-mm flares might also provide key information about the formation of hot onsets in solar flares (da Silva et al., 2023; Hudson et al., 2021).

Figure 2 .
Figure 2. Evolution of a synthetic sub-mm and IR flare T b spectrum from RHD modelling (from Simões et al., 2017).From these simulations, for λ > 50µm, T b should provide the electron temperature in the optically-thick upper chromosphere.
2).In addition to serendipitous detection as a by-product of other observations and surveys, dedicated stellar observations are essential for understanding the structure and activity of stellar atmospheres in general.The sample by Mohan et al. (2021) demonstrates the potential of stellar mm observations and, at the same time, illustrates the scarcity of suitable observations.AtLAST could make substantial contributions in this regard, either through targeted observations or also through coincidental (or even archival) detections.In particular, observations of stellar flares in the (sub-)mm range are extremely rare (MacGregor et al., 2018; MacGregor et al., 2020), and yet are crucial for unveiling the physics of these events including particle acceleration and plasma heating and for evaluating the impact of flares on the habitability of exoplanets (see, e.g., Bellotti et al., 2023; Konings et al., 2022; Lammer et al., 2003; Segura et al., 2010, and references therein).At millimeter wavelengths, the flux density of the few detected stellar flares tends to be 10 -1000 times higher than the quiescent flux.Assuming a typical quiet chromospheric temperature of ∼ 10 4 K (at 100 GHz) as seen in cool stars (Mohan et al., 2021), the flux density during a flare can vary in the range ∼ 0.5 -50 mJy for a star at a distance of 10 pc.It is important to emphasise that the flux varies

Figure 3 .
Figure 3.The ALMA sunspot mosaic (left) that was taken during the ALMA SV campaign on December 18, 2015 in Band 6 (230 GHz) at original interferometric resolution (left) and after convolution with the expected AtLAST beam (right).For reference, the ALMA single-dish beam (dashed line) and the AtLAST beam (solid line) are plotted in the lower left corner.
Fast on-the-fly scanning techniques (with a single beam) are used for creating maps of the whole solar disk or limited regions by, e.g, ALMA (White et al., 2017), and could be implemented for AtLAST, too (Kirkaune et al. in prep.).The scanning motion could be accomplished by moving the primary or secondary reflector.Scanning the whole disk with an ALMA TP antenna in a double-circle pattern (Phillips et al., 2015) takes on the order of 10 min.See Figure1for examples.

Figure 4 .
Figure 4. Left: AtLAST beam diameter as a function of observing frequency.The vertical dashed lines mark frequencies of 90 GHz and 660 GHz.Right: The resulting diameter of the instantaneous FOV as a function of number of detector pixels and observing frequency (see color legend).The resulting ratio of the FOV area and the whole disk of the Sun is overlaid as red contours.The dashed lines mark selected frequencies and detector numbers for reference.The pixels are assumed to have the size of the corresponding beam and are packed into a circle with no overlap.See Section 3.3 for details.
See the Solar ALMA Science Archive (SALSA, Henriques et al., 2022) for examples.Solar observations with AtLAST will be no different.The idea behind the suggested synoptic full-disk observations (see Section 3.2.1) is to provide a reference for complementary observations and to become a cornerstone of future solar observations very much like SDO today.The development of AtLAST can be fundamental to cover key ranges of the sub-mm spectrum for joint flare observations, along with instruments already in operation, such as the 30 THz cameras at Mackenzie University in São Paulo and at CASLEO, Argentina (Kudaka et al., 2015), the new High Altitude THz Solar photometer at 15 THz (HATS, Giménez de Castro et al., 2020) and future telescopes, such as the Solar Submillimeter Telescope Next Generation (SSTng, Giménez de Castro et al., 2023).
) "and thus contributing to the solution of many open questions (see Wedemeyer et al., 2016, and references therein)."This sentence appears to be vague.Perhaps a few examples of key science questions addressed would be instructive to the reader.

3 . 7 ,
Page first column, second paragraph;The Carrington event has an energy of the same order of magnitude as the 1e32 erg described in the same paragraph ( ~5e31 erg, e.g.) How much stronger (in orders of magnitude) are solar flares expected to be? puts the limit at ~1e36 for flares in general.

17 . 18 . 19 .
Page 12, first column, second paragraph; "...the 1.5m-aperture Solar Submillimeter Telescope (SST).." This telescope has already been introduced in the first paragraph of section 2.4, although without the citation.Page 12, first column, second paragraph; Perhaps a figure could be added of the FAL-C model (temperature vs height) and the approximate heights at which the telescope different bands are sensitive be marked.Page 13, first column, first paragraph; ToO -> undefined acronym 20.
prominence oscillations during a flare on AD Leonis.Astronomy and Astrophysics.1993; 274: 245-264 Reference Source 23.Gunn A.G., Doyle J.G., Mathioudakis M., Houdebine E.R., et al.: High-velocity evaporation during a flare on AT Microscopii.Astronomy and Astrophysics.1994; 285: 489-496 Reference Source 24.Guenther E.W., Emerson J.PR.: Spectrophotometry of flares and short time scale variations in weak line, and classical T Tauri stars in Chamaeleon.Astronomy and Astrophysics.1997; 321: 803-810 Reference Source 25.Fuhrmeister B, Schmitt J: Detection and high-resolution spectroscopy of a huge flare on the old M 9 dwarf DENIS 104814.7-395606.1.Astronomy & Astrophysics.2004; 420 (3): 1079-1085 Publisher Full Text 26.Vida K, Kriskovics L, Oláh K, Leitzinger M, et al.: Investigating magnetic activity in very stable stellar magnetic fields.Astronomy & Astrophysics.2016; 590.Publisher Full Text 27.Argiroffi C, Reale F, Drake J, Ciaravella A, et al.: A stellar flare−coronal mass ejection event revealed by X-ray plasma motions.Nature Astronomy.2019; 3 (8): 742-748 Publisher Full Text 28.Namekata K, Maehara H, Honda S, Notsu Y, et al.: Probable detection of an eruptive filament from a superflare on a solar-type star.Nature Astronomy.2021; 6 (2): 241-248 Publisher Full Text 29.Veronig A, Odert P, Leitzinger M, Dissauer K, et al.: Indications of stellar coronal mass ejections through coronal dimmings.Nature Astronomy.2021; 5 (7): 697-706 Publisher Full Text Is the background of the case's history and progression described in sufficient detail?Yes Is the work clearly and accurately presented and does it cite the current literature?Partly If applicable, is the statistical analysis and its interpretation appropriate?Not applicable Are all the source data underlying the results available to ensure full reproducibility?Not applicable Are the conclusions drawn adequately supported by the results?Yes Is the case presented with sufficient detail to be useful for teaching or other practitioners?Partly Competing Interests: No competing interests were disclosed.
et al., 2018; Heinzel et al., 2022; Labrosse et al., 2022; Menezes et al., 2022; Oliveira e Silva et al., 2022; Rodger et al., 2019; Selhorst et al., 2019; Shimojo et al., 2017a; Skokić et al., 2023; Valle Silva et al., This is an open access peer review report distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Chintzoglou et al. 2021 I & II [references 1,2].Could I ask the authors comment on the findings stated in the summary and conclusions of Chintzoglou et al. 2021 II, regarding the discrepancy between the formation heights of Band 6 found in this study and earlier ones.Do you believe that discussion of formation height for different solar features have already been resolved clearly to the satisfaction of the community?If not what are the knock-on error bars like for the key science cases based on these uncertainties or disagreements?(4) "Despite already large success of ALMA in advancing solar physics (e.g.Brajša et al., 2018; Heinzel et al., 2022; Labrosse et al., 2022; Menezes et al., 2022; Oliveira e Silva et al., 2022; Rodger et al., 2019; Selhorst et al., 2019; Shimojo et al., 2017a; Skokić et al., 2023; Valle Silva et al., 2021),there are important science cases that require different observational capabilities" I recommend that you split these advances into a few themes and at least mention what themes these are that ALMA has advanced.It's the second claim in the introduction of big contributions to advancements in the field with no specific examples yet provided to the reader.Further interesting advances from authors not associated with this work also perhaps warrant consideration in such a list.for example Multiple papers by Da Silva Santos, Chinzoglou, Molnar spring to mind, but there are also others [references 1-8].I am not requesting an in-depth discussion or an exhaustive list, but some context for the reader who is not familiar with these works.

Is the background of the case's history and progression described in sufficient detail? Yes Is the work clearly and accurately presented and does it cite the current literature? Partly If applicable, is the statistical analysis and its interpretation appropriate? Not applicable Are all the source data underlying the results available to ensure full reproducibility? Not applicable Are the conclusions drawn adequately supported by the results? Yes Is the case presented with sufficient detail to be useful for teaching or other practitioners? Partly Competing Interests:
Combining data from circular scans (if possible on a second time scale or at least <10 s) would then allow to produce data with higher angular resolution.A detailed study is currently in preparation (Kirkaune et al. in prep.)."Have the matters been studied in detail, or are being studied in detail (in prep)?If the former, I would recommend an additional citation to a published work referenced in first part of this paragraph.Region Filament With ALMA and IRIS.Frontiers in Astronomy and Space Sciences.2022; 9. Publisher Full Text 7. Molnar M, Reardon K, Chai Y, Gary D, et al.: Solar Chromospheric Temperature Diagnostics: A Joint ALMA-Hα Analysis.The Astrophysical Journal.2019; 881 (2).Publisher Full Text 8. Molnar M, Reardon K, Cranmer S, Kowalski A, et al.: High-frequency Wave Power Observed in the Solar Chromosphere with IBIS and ALMA.The Astrophysical Journal.2021; 920 (2).Publisher Full Text 9. Pietrow A, Kiselman D, de la Cruz Rodríguez J, Díaz Baso C, et al.: Inference of the chromospheric magnetic field configuration of solar plage using the Ca II 8542 Å line.Astronomy & Astrophysics.2020; 644.Publisher Full Text 10.Morosin R, de la Cruz Rodríguez J, Díaz Baso C, Leenaarts J: Spatio-temporal analysis of chromospheric heating in a plage region.Astronomy & Astrophysics.2022; 664.Publisher Full Text 11.Vissers G, Danilovic S, de la Cruz Rodríguez J, Leenaarts J, et al.: Non-LTE inversions of a confined X2.2 flare.Astronomy & Astrophysics.2021; 645.Publisher Full Text No competing interests were disclosed.

Is the background of the case's history and progression described in sufficient detail? Yes Is the work clearly and accurately presented and does it cite the current literature? Yes If applicable, is the statistical analysis and its interpretation appropriate? Not applicable Are all the source data underlying the results available to ensure full reproducibility? Not applicable Are the conclusions drawn adequately supported by the results? Yes Is the case presented with sufficient detail to be useful for teaching or other practitioners? Yes
Competing Interests: No competing interests were disclosed.

Reviewer Expertise: Turbulence I confirm that I have read this submission and believe that I have an appropriate level of expertise to confirm that it is of an acceptable scientific standard.
This is an open access peer review report distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
. I have both comment types below in order of appearance.All comment locations are based on the PDF of the first version of the manuscript.
Page 6, second column, last paragraph; This paragraph should be more quantitative with examples and citations.